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Review of LIGO Upgrade Plans
Yuta MichimuraDepartment of Physics, University of Tokyo
April 13, 2017Ando Lab Seminar
• Introduction
• A+
• Voyager
• Cosmic Explorer
• Other issues on ISC
• Summary
• KAGRA+
Contents
2
• J. Miller +, PRD 91, 062005 (2015)
Prospects for doubling the range of Advanced LIGO
• B. Shapiro +, Cryogenics 81, 83 (2017)
Cryogenically cooled ultra low vibration silicon mirrors for
gravitational wave observatories
• B P Abbott +, CQG 34, 044001 (2017)
Exploring the sensitivity of next generation gravitational
wave detectors
• LSC, LIGO-T1500290
Instrument Science White Paper 2015
• LSC, LIGO-T1600119
The LSC-Virgo White Paper on Instrument Science (2016-
2017 edition)
References
3
GW Detectors in the World
4
USA Europe Japan
1G
2G
3G
LIGO(2002-2007)
Enhanced LIGO(2009-2010)
Advanced LIGO(2015-)
A+(2017?-)
Voyager(2025?-)
Cosmic Explorer(2035?-)
TAMA(1999-2004)
KAGRA(2020?-)
Virgo(2007-2011)
Advanced Virgo(2017?-)
Einstein Telescope(2030?-)
GEO(2002-2009)
GEO-HF(2009-)
KAGRA+(2024??-)
GW Detectors in the World
5
LIGO(2002-2007)
Enhanced LIGO(2009-2010)
Advanced LIGO(2015-)
A+(2017?-)
Voyager(2025?-)
Cosmic Explorer(2035?-)
TAMA(1999-2004)
KAGRA(2020?-)
Virgo(2007-2011)
Advanced Virgo(2017?-)
Einstein Telescope(2030?-)
GEO(2002-2009)
GEO-HF(2009-)
KAGRA+(2024??-)
USA Europe Japan
1G
2G
3G
• Ground motion
• Reduction method
- longer arms
- low frequency suspension
- multiple stage suspension
- site selection (underground, less human activities)
Seismic Noise
7
http://www.kinki-geo.co.jp/joujibidou.pdf
• Brownian motion of fibers
• Reduction method
- longer arms
- high Q material
- longer and thinner fiber
- cryogenic temperature
Suspension Thermal Noise
8
http://gwwiki.icrr.u-tokyo.ac.jp/JGWwiki/KAGRA
• Brownian motion of mirror surface coating
• Thermo-optic noise
- Thermo-refractive noise
thermal change in the refractive
index of the coating
- Thermo-elastic noise
thermal expansion of the coating
• Reduction method
- longer arms
- high Q material
- cryogenic temperature
- larger beam size
Coating Thermal Noise
9
Ta2O5
Ta2O5
Ta2O5
Ta2O5
SiO2
SiO2
SiO2
SiO2
interference
mirror substrate
• Quantum fluctuation of light
Radiation pressure noise Shot noise
• Reduction method
- longer arms
- interferometer configuration
(higher finesse, RSE, etc.)
- heavier mirrors
- squeezing
Quantum Noise
10
mirrorphotodiode
Laser
• Longer arms
Seismic, Suspension thermal, Coating thermal, Quantum
• Better suspension
Seismic
• Underground
Seismic
• Lager mirror (allows larger beam size)
Suspension thermal, Coating thermal, Quantum
• High Q material
Suspension thermal, Coating thermal
• Cryogenic temperature
Suspension thermal, Coating thermal
• Squeezing
Quantum
Summary of Noise Reduction
11
• Modest cost upgrade of aLIGO (< $10M-20M)
• Factor of 2 improvement in sensitivity
quantum noise
coating thermal noise
• Two stages
- frequency dependent squeezing
(after O2, 2017)
- better coating, possibly low-risk changes to suspensions
(after O3, 2018-2019)
• Also as risk reduction for aLIGO
- squeezing in case high power is difficult
- improved coating in case coating thermal noise is
underestimated
• Heavier mass, improved suspension for lower thermal noise
-> little impact on the astrophysical output
Advanced LIGO+ (A+)
14
reduce gas damping,
improve bounce and roll damping,
mitigate parametric instabilities, etc.
• Frequency dependent squeezing with 16m long filter cavity
(4km filter cavity is not required if no change in other noises)
• Coating thermal noise
AlGaAs crystalline coating not demonstrated with
40cm-scale mirror
• Heavier mass not feasible
400kg and 1m diameter fused silica possible
Polishing with Ion Beam Figuring up to 50cm possible
Coating up to 40cm possible (CSIRO),
LMA planning to scale-up
• Suspension thermal noise -> little impact
longer fiber, higher stress
heat treatment of fibers to reduce surface losses
modify geometry
A+ Details
15
• Benefit of each improvement assuming all other
improvements (6 dB) have already been made
Relative importance of upgrades
16
Quantum and Coating thermal
have largest effect up to 6 dB
4km filter cavity is effective
when other noises are reduced
Suspension thermal
have small impact
LIGO-T1600119
• 16 m filter cavity, 6 dB measured squeezing, 1/2 loss in
coating high refractive index layer
A+ Nominal Noise Budget
17LIGO-T1600119
• 4 km filter cavity, 8 dB measured squeezing, 1/4 loss in
coating high refractive index layer
A+ Optimistic Noise Budget
18LIGO-T1600119
• Mode matching, alignment control (OMC, filter cavity,
squeezed light source)
• Newtonian noise subtraction
• Better ISI (Internal Seismic Isolation)
improved vertical inertial sensor, improved position sensors
to reduce RMS motion of ISI
• Stray light control
• Arm length stabilization system
reduce complexity (possibly inject green from vertex)
• Optical coating quality
to reduce scattering
• Charge mitigation
• PSL design to minimize noise couplings
• Larger BS
Other R&Ds
19
• K. Goda+, Nature Physics 4, 472 (2008)
Squeezing with prototype SRMI
• LSC, Nature Physics 7, 962 (2011)
Squeezing with GEO600
• J. Aasi+, Nature Photonics 7, 613 (2013)
Squeezing with LHO
• E. Oelker+, PRL 116, 041102 (2016)
2 m filter cavity at 1.2 kHz
• A. R. Wade+, Scientific Reports 5, 18052 (2015)
• E. Oelker+, Optica 7, 682 (2017)
~1mrad phase noise with OPO
under high vacuum
• 16 m filter cavity prototype
at MIT on going
Experimental Demonstrations
20
• Major upgrade within existing facility
• Factor of 3 increase in BNS range (~1100Mpc)
• 200 kg Silicon, 123 K
• 200 W laser at 2 um
wavelength could be 1.55-2.1 um- silicon absorption
- stable high power laser
- quantum efficiency of PDs for squeezing
(high for 1064 and 1550 nm)
- wide angle scatter loss 1/λ2
• Shin-Etsu will make 45 cm dia. mCZ
(magnetic field applied Czochralski)
• amorphous Si/SiO2 coating
• see LIGO-T1400226
Voyager
22R. X. Adhikari, GWADW2017
• 300m filter cavity, 10 dB squeezing
Voyager Noise Budget
23LIGO-T1600119
worse than A+ ?
• 123 K for zero thermal expansion
thermoelastic noise, minimize RoC change
• Radiative cooling (no conductive heat path needed)
5 W heat extraction
• Movable heat link for initial cool down
Cryogenic Layout
24B. Shapiro +, Cryogenics 81, 83 (2017) & LIGO-T1400226
• Demonstrated
low temperature
and
low vibration
can be realized
Stanford Experiment
25B. Shapiro +, Cryogenics 81, 83 (2017)
• Mirror reached 121 K
Stanford Experiment
26B. Shapiro +, Cryogenics 81, 83 (2017) Liquid nitrogen ran out
• Inner shield displacement meets
the requirement (from scattering)
Stanford Experiment
27B. Shapiro +, Cryogenics 81, 83 (2017)
• Cryogenic system is not impacting the vibration isolation of
the mirror
Stanford Experiment
28B. Shapiro +, Cryogenics 81, 83 (2017)
Displacement of
vibration isolation table
• New facility
• BNS range beyond z=1 (~4 Gpc)
• Adapt A+ and Voyager technology to much longer arms
• Or, shorter baseline designs with breakthroughs in
- Newtonian noise cancellation
- coating and mechanical system engineering
- quantum non demolition interferometry
• Long life time (~50 years)
• On the surface or underground
1-10 Hz sensitivity in terms of
science/dollar
• L-shape or triangular shape
polarizations
Cosmic Explorer
30
• Quantum noise (fixed cavity pole)
• Coating thermal noise (fixed cavity geometry; w∝L)
• Suspension thermal noise and seismic noise
vertical noise coupling linearly increases with length
(due to the curvature of the Earth)
Longer Arms
31
Coating thickness and beam size grow with wavelength but the effects cancel
Hidden dependence: longer arms require larger mass because of larger beam
B P Abbott +, CQG 34, 044001 (2017)
• From Hongo Campus to Hachioji
40 km
32
• Based on Voyager technology (Silicon, 123 K, 1550 um)
CE Optimistic Noise Budget
33LIGO-T1600119
• Based on A+ technology, conservative coating improvement
CE Pessimistic Noise Budget
34LIGO-T1600119
• Essentially all compact binary coalescence in the universe
for z>20 mass range
Astrophysical Reach
35LIGO-T1600119
• Vibration noise from heat links
suspension point interferometer ?
• Improve robustness of the arm length stabilization system
inject green from vertex ?
• High power photo-detection
• Mode matching of output mode-cleaner (OMC)
interferometer thermal state
• Balanced homodyne detection for DARM
to allow for tunable homodyne readout angle
to avoid technical noises
• Sidles-Sigg instability
potential threat for Voyager/CE since higher power
angular control noise reduction ?
optical trapping of alignment ?
Other Issues (= Chances) on ISC 1
36
LIGO-T1600119
• Alignment sensing and control
OMC, squeezed light source, filter cavities ……
higher power, more higher order modes
band of GW detection moves down, but bandwidth
of alignment control increases (Sidles-Sigg)
• Thermal aberration sensing and control
modeling, wavefront sensors
• Fast data acquisition (increase sampling frequency)
• Adaptive noise cancellation, automatic optimization, modern
control
• Virtual interferometer (Simulated Plant)
• Mechanical simulation tool for vibration isolation system
automatically compute thermal noise
• Modelling thermal distortions and radiation pressure
Other Issues (= Chances) on ISC 2
37
LIGO-T1600119
Summary
38
• Integrated realistic studies, R&D experiments are ongoing
for LIGO upgradesLIGO-T1600119
(may be not scientifically exciting itself,
but necessary for big science)
Summary
39
• Integrated realistic studies, R&D experiments are ongoing
for LIGO upgradesLIGO-T1600119
KAGRA
3
23
Sapphire
23 K
23 K
35 cm Sap.
Fiber
55
290
1064
1
3.5 / 3.5
0
none
(may be not scientifically exciting itself,
but necessary for big science)
Summary
40
• Integrated realistic studies, R&D experiments are ongoing
for LIGO upgradesLIGO-T1600119
KAGRA
3
23
Sapphire
23 K
23 K
35 cm Sap.
Fiber
55
290
1064
1
3.5 / 3.5
0
none
(may be not scientifically exciting itself,
but necessary for big science)
• We should plan ahead (~10 years)
• Some R&D ongoing, but needs integrated study
- 300 m filter cavity experiment at NAOJ
- coating thermal noise experiment at NAOJ
- mirror absorption measurement at NAOJ
• Heat extraction vs suspension thermal noise
- thick short suspension is better for heat extraction
- thin long suspension is better for thermal noise
- lower the power ?
- less absorption ?
- half cryogenic ?
- 123 K ?
- ribbon ?
KAGRA+?
41http://gwwiki.icrr.u-tokyo.ac.jp/JGWwiki/KAGRA
Ribbon Suspension
42
E. Nishida, JGW-G1100558 (2011)
R. DeSalvo, JGW-G1201101 (2012)
whr
• Keep cross section
to keep heat extraction,
but move violin modes
to higher frequency
Sapphire vs Silicon
43
Yoichi Aso, JGW-G1000113 (slide from LCGT f2f meeting 2010)
• Gravitational-wave Advanced Sapphire Technology
GAST Proposal by LMA et al
44G. Cagnoli, 8th ET
Symposium (2017)
• Underground facility and serious cryogenic system (20 K)
are futuristic attractive infrastructure
• Filter cavity seems feasible, but adds more complexity
(alignment, mode matching, etc.)
• Heavier mass + frequency independent squeezing +
low power + cryogenic + underground
sounds simple for me
• Could be sapphire,
could be silicon
• R&D facility for heavier mass
cryogenic suspension,
mirror polish, coating ?
• Silicon prototype
interferometer ?
Random Thoughts
45